ﻻ يوجد ملخص باللغة العربية
The ANTARES neutrino telescope is presently being built in the Mediterranean Sea at a depth of 2500 m. The primary aim of the experiment is the detection of high energy cosmic muon neutrinos, which are identified by the muons that are produced in charged current interactions. These muons are detected by measuring the Cerenkov light which they emit traversing the detector. Sometimes a high momentum muon produces electromagnetic showers. The subject of this paper is a method to reconstruct these showers which includes several steps: an algorithm for the fit of the muon track parameters, preselection of detected photons belonging to a shower, and a final fit with the preselected detected photons to calculate the electromagnetic shower position. Finally a comparison between data obtained with that part of the detector that is currently in operation and simulations is presented.
The Baikal-GVD is a large scale neutrino telescope being constructed in Lake Baikal. The majority of signal detected by the telescope are noise hits, caused primarily by the luminescence of the Baikal water. Separating noise hits from the hits produc
Despite the significant experimental effort made in the last decades, the origin of the ultra-high energy cosmic rays is still largely unknown. Key astrophysical information to identify where these energetic particles come from is provided by their c
The Baikal Gigaton Volume Detector (Baikal-GVD) is a km$^3$-scale neutrino detector currently under construction in Lake Baikal, Russia. The detector consists of several thousand optical sensors arranged on vertical strings, with 36 sensors per strin
An algorithm is presented, that provides a fast and robust reconstruction of neutrino induced upward-going muons and a discrimination of these events from downward-going atmospheric muon background in data collected by the ANTARES neutrino telescope.
In this work, direct measurements of the muon density at $1000,textrm{m}$ from the shower axis obtained by the Akeno Giant Air Shower Array (AGASA) are analysed. The selected events have zenith angles $theta leq 36^{textrm{o}}$ and reconstructed ener